2,605 research outputs found
Neutral carbon and CO in 76 (U)LIRGs and starburst galaxy centers A method to determine molecular gas properties in luminous galaxies
We present fluxes in both neutral carbon [CI] lines at the centers of 76
galaxies with FIR luminosities between 10^{9} and 10^{12} L(o) obtained with
Herschel-SPIRE and with ground-based facilities, along with the J=7-6, J=4-3,
J=2-1 12CO and J=2-1 13CO line fluxes. We investigate whether these lines can
be used to characterize the molecular ISM of the parent galaxies in simple ways
and how the molecular gas properties define the model results. In most
starburst galaxies, the [CI]/13CO flux ratio is much higher than in Galactic
star-forming regions, and it is correlated to the total FIR luminosity. The
[CI](1-0)/CO(4-3), the [CI](2-1) (2-1)/CO(7-6), and the [CI] (2-1)/(1-0) flux
ratios are also correlated, and trace the excitation of the molecular gas. In
the most luminous infrared galaxies (LIRGs), the ISM is fully dominated by
dense and moderately warm gas clouds that appear to have low [C]/[CO] and
[13CO]/[12CO] abundances. In less luminous galaxies, emission from gas clouds
at lower densities becomes progressively more important, and a multiple-phase
analysis is required to determine consistent physical characteristics. Neither
the CO nor the [CI] velocity-integrated line fluxes are good predictors of H2
column densities in individual galaxies, and X(CI) conversion factors are not
superior to X(CO) factors. The methods and diagnostic diagrams outlined in this
paper also provide a new and relatively straightforward means of deriving the
physical characteristics of molecular gas in high-redshift galaxies up to z=5,
which are otherwise hard to determine
The excitation of near-infrared H2 emission in NGC 253
Because of its large angular size and proximity to the Milky Way, NGC 253, an
archetypal starburst galaxy, provides an excellent laboratory to study the
intricacies of this intense episode of star formation. We aim to characterize
the excitation mechanisms driving the emission in NGC 253. Specifically we aim
to distinguish between shock excitation and UV excitation as the dominant
driving mechanism, using Br\gamma, H_2 and [FeII] as diagnostic emission line
tracers. Using SINFONI observations, we create linemaps of Br\gamma,
[FeII]_{1.64}, and all detected H_2 transitions. By using symmetry arguments of
the gas and stellar gas velocity field, we find a kinematic center in agreement
with previous determinations. The ratio of the 2-1 S(1) to 1-0 S(1) H_2
transitions can be used as a diagnostic to discriminate between shock and
fluorescent excitation. Using the 1-0 S(1)/2-1 S(1) line ratio as well as
several other H_2 line ratios and the morphological comparison between H_2 and
Br\gamma and [FeII], we find that excitation from UV photons is the dominant
excitation mechanisms throughout NGC 253. We employ a diagnostic energy level
diagram to quantitatively differentiate between mechanisms. We compare the
observed energy level diagrams to PDR and shock models and find that in most
regions and over the galaxy as a whole, fluorescent excitation is the dominant
mechanism exciting the H_2 gas. We also place an upper limit of the percentage
of shock excited H_2 at 29%. We find that UV radiation is the dominant
excitation mechanism for the H_2 emission. The H_2 emission does not correlate
well with Br\gamma but closely traces the PAH emission, showing that not only
is H_2 fluorescently excited, but it is predominately excited by slightly lower
mass stars than O stars which excite Br\gamma, such as B stars
On measuring the Tully-Fisher relation at
The evolution of the line width - luminosity relation for spiral galaxies,
the Tully-Fisher relation, strongly constrains galaxy formation and evolution
models. At this moment, the kinematics of z>1 spiral galaxies can only be
measured using rest frame optical emission lines associated with star
formation, such as Halpha and [OIII]5007/4959 and [OII]3727. This method has
intrinsic difficulties and uncertainties. Moreover, observations of these lines
are challenging for present day telescopes and techniques. Here, we present an
overview of the intrinsic and observational challenges and some ways way to
circumvent them. We illustrate our results with the HST/NICMOS grism sample
data of z ~ 1.5 starburst galaxies. The number of galaxies we can use in the
final Tully-Fisher analysis is only three. We find a ~2 mag offset from the
local rest frame B and R band Tully-Fisher relation for this sample. This
offset is partially explained by sample selection effects and sample specifics.
Uncertainties in inclination and extinction and the effects of star formation
on the luminosity can be accounted for. The largest remaining uncertainty is
the line width / rotation curve velocity measurement. We show that high
resolution, excellent seeing integral field spectroscopy will improve the
situation. However, we note that no flat rotation curves have been observed for
galaxies with z>1. This could be due to the described instrumental and
observational limitations, but it might also mean that galaxies at z>1 have not
reached the organised motions of the present day.Comment: 13 pages, 7 figures, A&A accepte
The spatial distribution of excited H_2 in T Tau: a molecular outflow in a young binary system
Strong extended emission from molecular hydrogen
in the v = 1 → 0 S(l) transition is mapped around T Tau. In
addition, the v = 2 → 1 S(l) line is detected close to the star. The ratio of the two transitions is consistent with an excitation process in which both fluorescence by stellar ultraviolet radiation and collisions in a warm, dense medium play a role. The morphology is interpreted as emission from a molecular outflow which appears to wiggle as a result of the fact that T Tau is a binary system seen almost pole-on. It is shown that an outflow with a small opening angle can reproduce the observed extended emission. From comparison with previous studies it is argued that the molecular outflow originates from T Tau S, the infrared component. The presented model constrains the orientation and geometry of the system
Molecular gas heating in Arp 299
Understanding the heating and cooling mechanisms in nearby (Ultra) luminous
infrared galaxies can give us insight into the driving mechanisms in their more
distant counterparts. Molecular emission lines play a crucial role in cooling
excited gas, and recently, with Herschel Space Observatory we have been able to
observe the rich molecular spectrum. CO is the most abundant and one of the
brightest molecules in the Herschel wavelength range. CO transitions are
observed with Herschel, and together, these lines trace the excitation of CO.
We study Arp 299, a colliding galaxy group, with one component harboring an AGN
and two more undergoing intense star formation. For Arp 299 A, we present PACS
spectrometer observations of high-J CO lines up to J=20-19 and JCMT
observations of CO and HCN to discern between UV heating and alternative
heating mechanisms. There is an immediately noticeable difference in the
spectra of Arp 299 A and Arp 299 B+C, with source A having brighter high-J CO
transitions. This is reflected in their respective spectral energy line
distributions. We find that photon-dominated regions (PDRs) are unlikely to
heat all the gas since a very extreme PDR is necessary to fit the high-J CO
lines. In addition, this extreme PDR does not fit the HCN observations, and the
dust spectral energy distribution shows that there is not enough hot dust to
match the amount expected from such an extreme PDR. Therefore, we determine
that the high-J CO and HCN transitions are heated by an additional mechanism,
namely cosmic ray heating, mechanical heating, or X-ray heating. We find that
mechanical heating, in combination with UV heating, is the only mechanism that
fits all molecular transitions. We also constrain the molecular gas mass of Arp
299 A to 3e9 Msun and find that we need 4% of the total heating to be
mechanical heating, with the rest UV heating
Periodic bursts of Star Formation in Irregular Galaxies
We present N-body/SPH simulations of the evolution of an isolated dwarf
galaxy including a detailed model for the ISM, star formation and stellar
feedback. Depending on the strength of the feedback, the modelled dwarf galaxy
shows periodic or quasi-periodic bursts of star formation of moderate strength.
The period of the variations is related to the dynamical timescale, of the
order of yr. We show that the results of these simulations are in
good agreement with recent detailed observations of dwarf irregulars (dIrr) and
that the peculiar kinematic and morphological properties of these objects,as
revealed by high resolution HI studies, are fully reproduced. We discuss these
results in the context of recent surveys of dwarf galaxies and point out that
if the star formation pattern of our model galaxy is typical for dwarf
irregulars this could explain the scatter of observed properties of dwarf
galaxies. Specifically, we show that the time sampled distribution of the ratio
between the instanteneous star formation rate (SFR) and the mean SFR is similar
to that distribution in observed sample of dwarf galaxies.Comment: 11 pages, 6 figures, accepted for A&
The Elusive Active Nucleus of NGC 4945
We present new HST NICMOS observations of NGC 4945, a starburst galaxy
hosting a highly obscured active nucleus that is one of the brightest
extragalactic sources at 100 keV. The HST data are complemented with ground
based [FeII] line and mid--IR observations. A 100pc-scale starburst ring is
detected in Pa alpha, while H_2 traces the walls of a super bubble opened by
supernova-driven winds. The conically shaped cavity is particularly prominent
in Pa alpha equivalent width and in the Pa alpha/H_2 ratio. Continuum images
are heavily affected by dust extinction and the nucleus of the galaxy is
located in a highly reddened region with an elongated, disk-like morphology. No
manifestation of the active nucleus is found, neither a strong point source nor
dilution in CO stellar features, which are expected tracers of AGN activity.
Even if no AGN traces are detected in the near-IR, with the currently available
data it is still not possible to establish whether the bolometric luminosity of
the object is powered by the AGN or by the starburst: we demonstrate that the
two scenarios constitute equally viable alternatives. However, the absence of
any signature other than in the hard X-rays implies that, in both scenarios,
the AGN is non-standard: if it dominates, it must be obscured in all
directions, conversely, if the starburst dominates, the AGN must lack UV
photons with respect to X-rays. An important conclusion is that powerful AGNs
can be hidden even at mid-infrared wavelengths and, therefore, the nature of
luminous dusty galaxies cannot be always characterized by long-wavelength data
alone but must be complemented with sensitive hard X-ray observations.Comment: Accepted for publication in A&A, high quality color pictures
available at http://www.arcetri.astro.it/~marconi/colpic.htm
Star Formation in Extreme Environments: The Effects of Cosmic Rays and Mechanical Heating
Context: Molecular data of extreme environments, such as Arp 220, but also
NGC 253, show evidence for extremely high cosmic ray (CR) rates (10^3-10^4 *
Milky Way) and mechanical heating from supernova driven turbulence.
Aims: The consequences of high CR rates and mechanical heating on the
chemistry in clouds are explored.
Methods: PDR model predictions are made for low, n=10^3, and high, n=10^5.5
cm^-3, density clouds using well-tested chemistry and radiation transfer codes.
Column densities of relevant species are discussed, and special attention is
given to water related species. Fluxes are shown for fine-structure lines of O,
C+, C, and N+, and molecular lines of CO, HCN, HNC, and HCO+. A comparison is
made to an X-ray dominated region model.
Results: Fine-structure lines of [CII], [CI], and [OI] are remarkably similar
for different mechanical heating and CR rates, when already exposed to large
amounts of UV. HCN and H2O abundances are boosted for very high mechanical
heating rates, while ionized species are relatively unaffected. OH+ and H2O+
are enhanced for very high CR rates zeta > 5 * 10^-14 s^-1. A combination of
OH+, OH, H2O+, H2O, and H3O+ trace the CR rates, and are able to distinguish
between enhanced cosmic rays and X-rays.Comment: 13 pages, 8 figures, A&A accepte
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